By Alan H. Batten (auth.), Alan H. Batten (eds.)
When leaving the Victoria airport the day earlier than our Colloquium, I observed a van of the Dunsmuir inn marked with mammoth letters which I learn as "Alcohol Colloquium". I do frequently make such error as a result worldwide, informal, and careless approach within which I learn quite a few advertisements, and checked myself speedy to learn it safely as "Algol Colloquium". thousands of fellow voters might simply make a similar mistake, and no apology may be anticipated. Even I learn and listen to the notice alcohol extra usually than Algol, even if i need to say that Algols have given me extra excitement and less complications through the years; in that, in spite of the fact that, i'll be a singularity, and probably a pitiful one at that. Being appointed Chairman of the medical Organizing Committee, i'll be deemed to be a purer" Algolist" than different investigators, even if my diversity of lively pursuits is far broader; and an identical is right approximately the entire 28 invited audio system and all of the different individuals of the Colloquium. Our curiosity are strongly diverse, yet there are numerous stable purposes that introduced us jointly at this Colloquium.
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Additional info for Algols: Proceedings of the 107th Colloquium of the International Astronomical Union held in Sidney, B.C., Canada, August 15–19, 1988
OLSON 30 ... 0 , ". • •• • :•. , '. " '\ I . I '':f, ~ ~ •. 00 Orbital Phose Fig. 1. Yellow observations of KU Cyg, mostly outside primary eclipse, obtained from 1982 to 1987. Four-point running normals are plotted. 5 is due to a slow, quasicyclical brightness variation of the entire system, similar to the variation seen in RX Cas. 0 • 0. o I. , " .... I -. '" I .... ~ WD 1 • ! 0 Orbital Phose Fig. 2. Infrared observations of KU Cyg, with the slow variation shifted out. 0, where the observer sees the region where stream and disk interact.
Perhaps not surprisingly, a parabolic fit to these observations reduces the predicted mean error per point by about 20%, relative to the linear ephemeris. This fit implies a period change dP/P z -2xlO- 7 which is at least of the correct sign for the proposed effect. Unfortunately, many years will pass before proof of a period decrease and its magnitude can be found. If this view of shock dissipation in the leading half of the disk is correct, then it is not surprising that emission and light-blocking have different radial distributions in the disk.
CONCLUSIONS Some of the characteristics of the disks in selected Algol disks implied by this investigation are enumerated in Table 1. For each system, its period, phases at which disk occultation begin/ends (¢V, ¢R), the estimated radial extent of the disk relative to the size of the primary's Roche surface (Rd/~p), and comments on whether any asymmetry in brightness has been observed are given. The conclusions from this study can be summarized as follows: 1. The presence and stability of an Het emitting accretion disk appear to depend on the location of the system in the r-q diagram (Fig.